scholarly journals A statistical study into the spatial distribution and dawn-dusk asymmetry of dayside magnetosheath ion temperatures as a function of upstream solar wind conditions

2015 ◽  
Vol 120 (4) ◽  
pp. 2767-2782 ◽  
Author(s):  
A. P. Dimmock ◽  
K. Nykyri ◽  
H. Karimabadi ◽  
A. Osmane ◽  
T. I. Pulkkinen
Keyword(s):  
Solar Wind ◽  
Spatial Distribution ◽  
Statistical Study ◽  
Upstream Solar Wind

Solar Wind Interaction With Jupiter's Magnetosphere: A Statistical Study of Galileo In Situ Data and Modeled Upstream Solar Wind Conditions

2019 ◽  
Vol 124 (12) ◽  
pp. 10170-10199 ◽  
Author(s):  
Marissa F. Vogt ◽  
Szilard Gyalay ◽  
Elena A. Kronberg ◽  
Emma J. Bunce ◽  
William S. Kurth ◽  
...  
Keyword(s):  
Solar Wind ◽  
Statistical Study ◽  
Solar Wind Interaction ◽  
In Situ Data ◽  
Upstream Solar Wind

Subsolar magnetopause under an inverse gradient of the magnetic field: Statistical study

2020 ◽  
Author(s):  
Kostiantyn Grygorov ◽  
Zdeněk Němeček ◽  
Jana Šafránková ◽  
Jiří Šimůnek
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Thermal Plasma ◽  
Statistical Study ◽  
The State ◽  
Upstream Solar Wind ◽  
The Magnetic Field

<p>The magnetopause is usually at the point where the pressure of the magnetospheric magnetic field is balanced by a sum of the thermal plasma and magnetic pressures on the magnetosheath side. However, statistics from THEMIS magnetopause crossings have showed that about 2 % of them exhibit a larger magnetic field in the magnetosheath than in the magnetosphere in the subsolar region (Y<sub>GSM </sub>< 5 R<sub>E</sub>) and thus, the pressure from the magnetosheath side seems to be uncompensated. In our study, we compare parameters of those unusual crossings with the rest of our statistic in that region with motivation to highlight the possible sources and mechanisms of this apparent pressure imbalance, which can be caused either by specific upstream solar wind conditions or by the state of the magnetosphere. We also compare our THEMIS results with the sets of magnetopause crossings observed by other spacecraft (e.g., Cluster, MMS).</p>

Statistical study of the effect of solar wind dynamic pressure fronts on the dayside and nightside ionospheric convection

2011 ◽  
Vol 116 (A10) ◽  
pp. n/a-n/a ◽  
Author(s):  
A. Boudouridis ◽  
L. R. Lyons ◽  
E. Zesta ◽  
J. M. Weygand ◽  
A. J. Ribeiro ◽  
...  
Keyword(s):  
Solar Wind ◽  
Statistical Study ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Ionospheric Convection

scholarly journals Density holes in the upstream solar wind

2007 ◽  
Author(s):  
G. K. Parks ◽  
E. Lee ◽  
N. Lin ◽  
F. Mozer ◽  
M. Wilber ◽  
...  
Keyword(s):  
Solar Wind ◽  
Upstream Solar Wind

scholarly journals Remotely distinguishing and mapping endogenic water on the Moon

2017 ◽  
Vol 375 (2094) ◽  
pp. 20150391 ◽  
Author(s):  
Rachel L. Klima ◽  
Noah E. Petro
Keyword(s):  
Solar Wind ◽  
Spatial Distribution ◽  
Solar System ◽  
The Moon ◽  
Testing Hypotheses ◽  
Origin And Evolution ◽  
Lunar Interior ◽  
Geological Features ◽  
Insight Into

Water and/or hydroxyl detected remotely on the lunar surface originates from several sources: (i) comets and other exogenous debris; (ii) solar-wind implantation; (iii) the lunar interior. While each of these sources is interesting in its own right, distinguishing among them is critical for testing hypotheses for the origin and evolution of the Moon and our Solar System. Existing spacecraft observations are not of high enough spectral resolution to uniquely characterize the bonding energies of the hydroxyl molecules that have been detected. Nevertheless, the spatial distribution and associations of H, OH − or H 2 O with specific lunar lithologies provide some insight into the origin of lunar hydrous materials. The global distribution of OH − /H 2 O as detected using infrared spectroscopic measurements from orbit is here examined, with particular focus on regional geological features that exhibit OH − /H 2 O absorption band strengths that differ from their immediate surroundings. This article is part of the themed issue ‘The origin, history and role of water in the evolution of the inner Solar System’.

Statistical Study of the Effect of Different Solar Wind Types on Magnetic Storm Generation During 1995–2016

2018 ◽  
Vol 58 (6) ◽  
pp. 737-743 ◽  
Author(s):  
L. A. Dremukhina ◽  
I. G. Lodkina ◽  
Y. I. Yermolaev
Keyword(s):  
Solar Wind ◽  
Magnetic Storm ◽  
Statistical Study

Spatial distribution of turbulence characteristics in the inner solar wind

2010 ◽  
Vol 54 (5) ◽  
pp. 446-455 ◽  
Author(s):  
A. I. Efimov ◽  
L. A. Lukanina ◽  
L. N. Samoznaev ◽  
I. V. Chashei ◽  
M. K. Bird ◽  
...  
Keyword(s):  
Solar Wind ◽  
Spatial Distribution ◽  
Turbulence Characteristics

scholarly journals Foreshock cavitons and spontaneous hot flow anomalies: A statistical study with a global hybrid-Vlasov simulation

2021 ◽  
Author(s):  
Vertti Tarvus ◽  
Lucile Turc ◽  
Markus Battarbee ◽  
Jonas Suni ◽  
Xóchitl Blanco-Cano ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Rest Frame ◽  
Statistical Study ◽  
Plasma Temperature ◽  
Propagation Speed ◽  
Bow Shock ◽  
Ulf Waves ◽  
Subsequent Formation ◽  
Comparable Amount

Abstract. The foreshock located upstream of Earth's bow shock hosts a wide variety of phenomena related to the reflection of solar wind particles from the bow shock and the subsequent formation of ultra-low frequency (ULF) waves. In this work, we investigate foreshock cavitons, which are transient structures resulting from the non-linear evolution of ULF waves, and spontaneous hot flow anomalies (SHFAs), which evolve from cavitons as they accumulate suprathermal ions while being carried to the bow shock by the solar wind. Using the global hybrid-Vlasov simulation model Vlasiator, we have conducted a statistical study in which we track the motion of individual cavitons and SHFAs in order to examine their properties and evolution. In our simulation run where the interplanetary magnetic field (IMF) is directed at a sunward-southward angle of 45 degrees, continuous formation of cavitons is found up to ~ 11 Earth radii (RE) from the bow shock (along the IMF direction), and caviton-to-SHFA evolution takes place within ~ 2 RE from the shock. A third of the cavitons in our run evolve into SHFAs, and we find a comparable amount of SHFAs forming independently near the bow shock. We compare the properties of cavitons and SHFAs to prior spacecraft observations and simulations, finding good agreement. We also investigate the variation of the properties as a function of position in the foreshock, showing that the transients close to the bow shock are associated with larger depletions in the plasma density and magnetic field magnitude, along with larger increases in the plasma temperature and the level of bulk flow deflection. Our measurements of the propagation velocities of cavitons and SHFAs agree with earlier studies, showing that the transients propagate sunward in the solar wind rest frame. We show that SHFAs have a greater solar wind rest frame propagation speed than cavitons, which is related to an increase in the magnetosonic speed near the bow shock.

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